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One of the simplest ways to identify an exoplanetary transit is to phase folda photometric time series upon a trial period - leading to a coherent stackwhen using the correct value. Such phase-folded transits have become a standarddata visualisation in modern transit discovery papers. There is no analogousfolding mechanism for exomoons, which would have to represent some kind ofdouble-fold; once for the planet and then another for the moon. Folding withthe planet term only, a moon imparts a small decrease in the surroundingout-of-transit averaged intensity, but its incoherent nature makes it far lessconvincing than the crisp stacks familiar to exoplanet hunters. Here, a newapproach is introduced that can be used to achieve the transit origami neededto double fold an exomoon, in the case where a planet exhibits TTVs. Thisdouble fold has just one unknown parameter, the satellite-to-planet mass ratio,and thus a simple one-dimensional grid search can be used to rapidly identifypower associated with candidate exomoons. The technique is demonstrated onsimulated light curves, exploring the breakdown limits of close-in and/orinclined satellites. As an example, the method is deployed on Kepler-973b, awarm mini-Neptune exhibiting an 8 minute TTV, where the possibility that theTTVs are caused by a single exomoon is broadly excluded, with upper limitsprobing down to a Ganymede-sized moon.

Transit Origami: A Method to Coherently Fold Exomoon Transits in Time Series Photometry